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The wide-binary origin of (2014) MU_(69)-like Kuiper belt contact binaries

机译：（2014）MU_（69）型柯伊伯带接触二进制的宽二进制起源

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Following its flyby and first imaging of the Pluto-Charon binary, the New Horizons spacecraft visited the Kuiper belt object (KBO) 2014 MU69 (also known as (486958) Arrokoth). The imaging showed MU69 to be a contact binary that rotates at a low spin period (15.92 hours), is made of two individual lobes connected by a narrow neck and has a high obliquity (about 98 degrees)(1), properties that are similar to those of other KBO contact binaries inferred through photometric observations(2). However, all scenarios suggested so far for the origins of such configurations(3-5) have failed to reproduce these properties and their probable frequent occurrence in the Kuiper belt. Here we show that semi-secular perturbations(6,7) operating on only ultrawide KBO binaries close to their stability limit can robustly lead to gentle, slow binary mergers at arbitrarily high obliquities but low rotational velocities, reproducing the characteristics of MU69 and other similar oblique contact binaries. Using N-body simulations, we find that approximately 15 per cent of all ultrawide binaries with a cosine-uniform inclination distribution(5,9) are likely to merge through this process. Moreover, we find that such mergers are sufficiently gentle to deform the shape of the KBO only slightly. The semi-secular contact binary formation channel not only explains the observed properties of MU69, but may also apply to other Kuiper belt or asteroid belt binaries and in the Solar System and extra-solar moon systems.The high obliquity and low rotation period of the Kuiper belt object (2014) MU69 and other similar contact binaries is successfully reproduced from the collision and post-collision characteristics of initially wide binaries.
机译：飞越并首次对冥王星-夏隆双星成像后，新视野号航天器访问了柯伊伯带天体（KBO）2014 MU69（也称为（486958）Arrokoth）。成像显示MU69是一个在低自旋周期（15.92小时）旋转的接触二元体，由两个狭窄的脖子相连的单个裂片组成，并具有很高的倾角（大约98度）（1），性质相似与通过光度法观察得出的其他KBO接触式二进制文件的结果（2）。但是，到目前为止，对于这种构造的起源（3-5）提出的所有方案都未能重现这些性质，并且它们可能在柯伊伯带中频繁发生。在这里我们表明，仅在接近其稳定极限的超宽KBO二进制上运行的半长期扰动（6,7）可以在任意高的倾斜度但较低的旋转速度下稳健地导致缓慢，缓慢的二进制合并，从而再现了MU69和其他类似特征斜接触二进制文件。使用N体模拟，我们发现在整个余弦均匀的倾角分布（5,9）的超宽二进制文件中，大约有15％可能会在此过程中合并。此外，我们发现这种合并足够温和，仅会使KBO的形状发生轻微变形。半长期接触双星形成通道不仅解释了MU69的观测特性，而且还可能适用于其他柯伊伯带或小行星带双星以及太阳系和太阳系外月球系统。从最初较宽的二进制文件的碰撞和碰撞后特性成功复制了柯伊伯带天体（2014）MU69和其他类似的接触二进制文件。

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  • 来源
    《Nature》 |2020年第7804期|463-466|共4页
  • 作者

    Grishin Evgeni; Malamud Uri; Perets Hagai B.; Wandel Oliver; Schaefer Christoph M.;

  • 作者单位

    Technion Israel Inst Technol Phys Dept Haifa Israel;

    Eberhard Karls Univ Tubingen Inst Astron & Astrophys Tubingen Germany;

  • 收录信息 美国《科学引文索引》(SCI);美国《工程索引》(EI);美国《生物学医学文摘》(MEDLINE);美国《化学文摘》(CA);
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